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(145453) 2005 RR43: a Case for a Carbon-Depleted Population of Tnos?

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(145453) 2005 RR43: a Case for a Carbon-Depleted Population of Tnos? A&A 468, L25–L28 (2007) Astronomy DOI: 10.1051/0004-6361:20077294 & c ESO 2007 Astrophysics Letter to the Editor The water ice rich surface of (145453) 2005 RR43: a case for a carbon-depleted population of TNOs? N. Pinilla-Alonso1, J. Licandro2,3, R. Gil-Hutton4, and R. Brunetto5,6 1 Fundación Galileo Galilei & Telescopio Nazionale Galileo, PO Box 565, 38700, S/C de La Palma, Tenerife, Spain e-mail: [email protected] 2 Isaac Newton Group, 38700 Santa Cruz de La Palma, Tenerife, Spain 3 Instituto de Astrofísica de Canarias, c/Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain 4 Complejo Astronómico El Leoncito (Casleo) and San Juan National University, Av. España 1512 sur, J5402DSP, San Juan, Argentina 5 Dipartimento di Fisica, Università del Salento, via Arnesano, 73100 Lecce, Italy 6 INAF-Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy Received 13 February 2007 / Accepted 23 April 2007 ABSTRACT Context. Recent results suggest that there is a group of trans-Neptunian objects (TNOs) (2003 EL61 being the biggest member), with surfaces composed of almost pure water ice and with very similar orbital elements. These objects provide exciting laboratories for the study of the processes that prevent the formation of an evolved mantle of organics on the surfaces of the bodies in the trans-Neptunian belt (TNb). Aims. We study the surface composition of another TNO that moves in a similar orbit, (145453) 2005 RR43, and compare it with the surface composition of the other members of the group. Methods. We report visible and near-infrared spectra in the 0.53−2.4 µm spectral range, obtained with the 4.2 m William Herschel Telescope and the 3.58 m Telescopio Nazionale Galileo at the “Roque de los Muchachos” Observatory (La Palma, Spain). Scattering models are used to derive information about its surface composition. We also measure the depth D of the water ice absorption bands and compare with those of the other members of the group. Results. The spectrum of 2005 RR43 is neutral in color in the visible and dominated by very deep water ice absorption bands in the near infrared (D = 70.3 ± 2.1% and 82.8 ± 4.9% at 1.5 µm and 2.0 µm respectively). It is very similar to the spectrum of the group of TNOs already mentioned. All of them present much deeper water ice absorption bands (D > 40%) than any other TNO except Charon. Scattering models show that its surface is covered by water ice, a significant fraction in crystalline state with no trace (5% upper limit) of complex organics. Possible scenarios to explain the existence of this population of TNOs are discussed: a giant collision, an originally carbon depleted composition, or a common process of continuous resurfacing. Conclusions. 2005 RR43 is member of a group, may be a population, of TNOs clustered in the space of orbital parameters that show abundant water ice and no signs of complex organics and which origin needs to be further investigated. The lack of complex organics in their surfaces suggests a significant smaller fraction of carbonaceous volatiles like CH4 in this population than in “normal” TNOs. A carbon depleted population of TNOs could be the origin of the population of carbon depleted Jupiter family comets already noticed by A’Hearn et al. (1995). Key words. Kuiper Belt – solar system: formation 1. Introduction (Brown et al. 1999) also have surface composition similar to Charon. During last year the spectra of five other objects were Spectroscopic and spectrophotometric studies show that published, revealing that their surfaces are also covered by fresh about 70% of TNOs present a mantle of complex organics on water ice: (136108) 2003 EL61 (Trujillo et al. 2007), its biggest their surfaces (Brunetto et al. 2006). Long term processing by satellite S/2005 (136108) 1 (Barkume et al. 2006) and during high energy particles and solar radiation on icy bodies, induces the review process of this paper 2003 OP32, 1995 SM55 and the formation of organic species in their outer layers, resulting in 2005 RR43 (Brown et al. 2007). The spectra of these TNOs show a mantle that covers the unprocessed original ices (Moore et al. all the same characteristics, they are neutral and featureless in the 1983; Johnson et al. 1984; Strazzulla & Johnson 1991). Until visible and show strong water ice absorption bands in the near recently, the only case of a TNO with a surface covered basically infrared. All these TNOs, except Charon, are located in a narrow by a thick layer of water ice was Charon (Buie et al. 1987; region of the orbital parameters space (41.6 < a < 43.6AU, Marcialis et al. 1987), and it has been considered an intringuing 25.8 < i < 28.2deg,0.10 < e < 0.19). The existence of a pop- case because of the need of a resurfacing mechanism like ulation of TNOs with Charon-like surfaces and similiar orbital cryovolcanism or collisons with micro-meteorites (Brown 2002; parameters needs to be explained as it can have a strong impact Cruikshank 1998). Recently, it has been showed that (55636) in the knowledge of the trans-neptunian belt formation theories 2002 TX300 (Licandro et al. 2006) and (13308) 1996 TO66 and/or resurfacing mechanisms. Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20077294 L26 N. Pinilla-Alonso et al.: The surface of (145453) 2005 RR43: a case for a carbon-depleted population of TNOs? In this paper we present visible and near-infrared spec- troscopy of a member of this group, (145453) 2005 RR43 (a, e, i = 43.06 AU, 0.14, 28.54 deg) and derive compositional information using scattering models. Finally we describe differ- ent scenarios that can explain the existence of this population of TNOs. 2. Observations and analysis of the spectrum We obtained the visible spectrum of 2005 RR43 with the 4.2 m William Herschel telescope (WHT) and the near-infrared spec- trum with the 3.58 m “Telescopio Nazionale Galileo” (TNG) both at the “Roque de los Muchachos” Observatory (Canary Islands, Spain). The visible spectrum (0.35−0.95 µm) was obtained on 2006 Sep. 23.18 UT using the low resolution grating (R158R, Fig. 1. Spectrum of 2005 RR43, normalized at 0.55 µm, together with with a dispersion of 1.63 Å/pixel) of the double-armed spectro- the spectra of the other members of the group shifted in the vertical axis graph ISIS at WHT, and a 4 slit width oriented at the parallactic for clarity. References in Table 1. angle. The tracking was at the TNO proper motion. Three 900 s exposure time spectra were obtained by shift- ing the object by 10 in the slit to better correct the fringing. the depth of the bands, D, with respect to the continuum of the Calibration and extraction of the spectra were done using IRAF = − / and following standard procedures (Massey et al. 1992). TNO spectrum as D 1 Rb Rc,whereRb is the reflectance in the spectra were averaged and the reflectance spectrum was obtained center of the band and Rc is the reflectance of the continuum at 1.2 µm. For 2005 RR43, D is 70.3 ± 2.1% and 82.8 ± 4.9% by dividing the spectrum of the TNO by the spectrum of the so- µ µ lar analogue star Hyades 64 obtained the same night just before at 1.5 m and 2.0 m respectively, beeing the deepest water ice and after the observation of the TNO at a similar airmass. Final absorption bands ever observed in a TNO. spectrum presented in Fig. 1 was smoothed using a smoothing Thus, we conclude that the surface of 2005 RR43 is com- box-car of 15 pixels to improve the S/N. posed by a large fraction of large sized (or a thick layer of) wa- The near-infrared spectrum was obtained on ter ice particles, and none or a very small fraction of complex 2006 Sep. 29.15 UT, using the low resolution spectroscopic organics or silicates. mode of NICS (Near-Infrared Camera and Spectrometer) at the This is confirmed by scattering models. We use the TNG based on an Amici prism disperser. This mode yields a simple one-dimensional geometrical-optics formulation by complete 0.8−2.4 µm spectrum. A 1.5 slit width corresponding Shkuratov et al. (1999), to obtain information about the surface to a spectral resolving power R 34 quasi-constant along the composition. spectrum was used. The observing and reduction procedures It is important to determine if water ice is in amorphous or were as described in Licandro et al. (2002). The total “on crystalline state as it can be indicative of resurfacing processes. object” exposure time was 11 160 s. Crystalline water ice can be easily identified by an absorption To correct for telluric absorption and to obtain the relative band at 1.65 µm. This band has been detected in the spec- reflectance, solar analogue star Hyades 64 and two G-2 Landolt trum of TNOs Charon (Brown & Calvin 2000) and 2003 EL61 stars (115−271 and 98−978, Landolt 1992) were observed at dif- (Trujillo et al. 2007), the only TNOs that have spectra similar ferent airmasses during the night. The reflectance spectrum of to 2005 RR43 and sufficiently high signal-to-noise to see this the TNO was obtained using all the SA stars, averaged and then band. Unfortunately, the relatively poor S/N of our spectrum normalized to fit the visible one using the overlapping spectral does not allow us to clearly detect this feature.
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